Anisotropic stars in gravity under class I space-time

S. K. Maurya; Ksh. Newton Singh; Abdelghani Errehymy; Mohammed Daoud

doi:10.1140/epjp/s13360-020-00832-8

EPJ

Anisotropic stars in

f (G, T)

$f({\textit{G}},{\textit{T}})$ gravity under class I space-time

S. K. Maurya¹^a, Ksh. Newton Singh², Abdelghani Errehymy³ and Mohammed Daoud⁴^,5

¹ Department of Mathematical and Physical Sciences, College of Arts and Science, University of Nizwa, Nizwa, Sultanate of Oman
² Department of Physics, National Defence Academy, 411023, Khadakwasla, Pune, India
³ Laboratory of High Energy Physics and Condensed Matter (LPHEMaC), Department of Physics, Faculty of Sciences Aïn Chock, Hassan II University of Casablanca, B.P. 5366 Maarif, 20100, Casablanca, Morocco
⁴ Department of Physics, Faculty of Sciences, University of Ibn Tofail, B.P. 133, 14000, Kenitra, Morocco
⁵ Abdus Salam International Centre for Theoretical Physics, 34151, Miramare, Trieste, Italy

Received: 22 August 2020
Accepted: 5 October 2020
Published online: 14 October 2020

Abstract

In this paper, we studied the possible existence of anisotropic spherically symmetric solutions in the arena of modified

f (G, T)

$f(\textit{G}, \textit{T})$ -gravity theory. To supply exact solutions of the field equations, we consider that the gravitational Lagrangian can be expressed as the generic function of the quadratic Gauss–Bonnet invariant

G

$\textit{G}$ and the trace of the stress–energy tensor

T

$\textit{T}$ , i.e.,

f (G, T) = G^{2} + χ T

$f(\textit{G},\textit{T}) = \textit{G}^2 + \chi \textit{T}$ , where

χ

$\chi$ is a coupling parameter. We ansatz the gravitational potential:

g_{rr} \equiv e^{λ (r)}

$g_{rr} \equiv e^{\lambda (r)}$ from the relationship quasi-local mass function,

e^{- λ} = 1 - \frac{2 m (r)}{r}

$e^{-\lambda }=1-\frac{2m(r)}{r}$ , and we obtained the gravitational potential:

g_{tt} \equiv e^{ν (r)}

$g_{tt} \equiv e^{\nu (r)}$ via the embedding class one procedure. In this regard, we investigated that the new solution is well analyzed and well comported through various physical and mathematical tests, which confirmed the physical viability and the stability of the system. The present investigation uncovers that the

f (G, T)

$f(\textit{G},\textit{T})$ -gravity via embedding class one approach is a well acceptable to describe compact systems, and we successfully compared the effects of all the necessary physical requirements with the standard results of

f (G)

$f(\textit{G})$ -gravity, which can be retrieved at

χ = 0

$\chi = 0$ .

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Anisotropic stars in $f (G, T)$ $f({\textit{G}},{\textit{T}})$ gravity under class I space-time

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Anisotropic stars in f(G,T) gravity under class I space-time

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Anisotropic stars in $f (G, T)$ $f({\textit{G}},{\textit{T}})$ gravity under class I space-time